Channeled propagation of slow magnetosonic waves in an inhomogeneous solar corona

Conference · Sun Dec 31 04:00:00 EST 1995

OSTI ID:226874

Mond, M; Rutkevich, I ^[1]

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1. Ben-Gurion Univ. of the Negev, Beer Sheva (Israel)

The propagation of magneto-acoustic waves in the atmosphere of the Sun is commonly associated with possible wave heating of the solar chromosphere and corona. The distributions of the magnetic field, the plasma density and the temperature in these regions do not posses a spherical symmetry and under certain conditions such nonuniformities may provide the localization of travelling magnetosonic waves near the magnetic field lines. In this note we draw attention to the localization of the slow magnetosonic waves (SMW) which can contribute to the creation of streamer-like structures of the solar corona. To illustrate this point of view we consider two-dimensional waves propagating in an axisymmetric cylindrical steady plasma configuration with a given axial magnetic field B = B(r)e{sub z}, and with given radial profiles of the temperature T(r) and the electron density n(r). It is assumed that the characteristic radial wavelength is much less than the characteristic length of plasma nonuniformity, so that the WKB method for calculating the wave solutions can be applied. In the framework of ideal magnetohydrodynamics (MHD), the two-dimensional axisymmetric solutions for small perturbations are sought.

• OSTI ID: 226874
• Report Number(s): CONF-950749--
• Country of Publication: United States
• Language: English

Related Subjects

66 PHYSICS
MAGNETOACOUSTIC WAVES
MAGNETOHYDRODYNAMICS
SOLAR CORONA
WAVE PROPAGATION